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Solar constant

About: Solar constant is a research topic. Over the lifetime, 967 publications have been published within this topic receiving 29647 citations.


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Journal ArticleDOI
TL;DR: The possible contributions of the SOHO to the solar terrestrial energy program are discussed in this article, where the authors discuss the contribution of SohO measurements and observations for the study of the energy flow in the solar terrestrial system: the total solar irradiance or solar constant will be monitored with an accuracy of about 0.15% by solar radiometers in one of the helioseismology instruments, the solar EUV irradiance will be measured directly by an EUV monitor (at 305 A) and obtained at several wavelength bands between 150 and 1600 A by integration
Abstract: The possible contributions of the SOHO to the Solar Terrestrial Energy Program are discussed. Several SOHO measurements and observations will be of interest for the study of the energy flow in the solar terrestrial system: - the total solar irradiance or solar constant will be monitored with an accuracy of about 0.15% by solar radiometers in one of the helioseismology instruments, - the solar EUV irradiance will be measured directly by an EUV monitor (at 305 A) and obtained at several wavelength bands between 150 and 1600 A by integration of spectroscopic images, - synoptic maps of the sun at different levels of the chromosphere, transition region and lower corona obtained in extreme ultra-violet (EUV) will be produced by the SOHO telescopes and spectrometers, - solar magnetograms with about 4 arc second resolution (2'' pixels) will be produced several times per day, - the evolution of the large coronal structures that shape the solar wind, as well as the coronal mass ejections will be followed by two coronagraphs and by a solar wind anisotropy measuring instrument; the latter generate the solar wind disturbances that are cause of the most energetic magnetic events in the geosphere, - the elemental, isotopic and charge state composition and energy distribution of the ions that form the solar wind, as well as of the energetic particles that will reach the earth magnetosphere, are determined in SOHO by a set of time-of-flight and solid state detectors.

2 citations

Journal ArticleDOI
TL;DR: In this paper, the ozone content from the long-term mean values for each station and then for all the stations, the final curve of the ozone trend shows agreement with the longterm variation of the solar constant (over the period from 1961-1992) which may be part of the 80-90 year Gleissberg cycle.

2 citations

Journal ArticleDOI
TL;DR: In this article, two definitions of solar intensity are discussed and it is shown that Wegener's definition, which includes Boltzmann-radiation of the instrument and the atmosphere, leads to conclusions opposite to representative measurements.
Abstract: Two definitions of solar intensity are discussed. It is shown, thatK. Wegener's definition, which includesBoltzmann-radiation of the instrument and the atmosphere, leads to conclusions opposite to representative measurements. The usual definition basing on energy-flux is proved by different methods and in very different climates. Yet there are still many problems to resolve before the solar constant will be known by an accuracy of ±1%.

2 citations

Journal ArticleDOI
TL;DR: Algebraic design equations were derived for an optical projection system that included lenticular plates and a collimating lens that produced an irradiance of 100 solar constants that was uniform to 1% within the volume of space occupied by a test model whose dimensions were of the order of 10 cm.
Abstract: Algebraic design equations were derived for an optical projection system that included lenticular plates and a collimating lens. The system was applied to a solar simulator using a 20-kW xenon lamp. It produced an irradiance of 100 solar constants that was uniform to 1% within the volume of space occupied by a test model whose dimensions were of the order of 10 cm.

2 citations

Book ChapterDOI
01 Jan 2014
TL;DR: In this article, the authors describe how leaves intercept the Sun's rays using the direct-beam solar radiation equation and apply it to the sloping surface of a leaf, showing how to use the equation to determine light interception on a leaf.
Abstract: This chapter describes how leaves intercept the Sun's rays. To understand the process, basic principles of astronomy are presented. Sidereal time, solar time, apparent solar time, mean solar time, and standard time are defined. The procedure for determining standard time from apparent solar time is given. Interception of direct-beam solar radiation then is discussed. It is based on the direct-beam solar radiation equation that has been in the literature for over 200 years. It can be used on any sloping surface, but in this chapter we apply it to the sloping surface of a leaf. Four angles need to be known to solve the equation: azimuth and altitude angle of the Sun and azimuth and altitude angle of the leaf. An example is given showing how to use the equation to determine light interception on a leaf. An appendix gives the biography of Kepler, whose work laid the foundation for astronomy.

2 citations


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Performance
Metrics
No. of papers in the topic in previous years
YearPapers
20238
202215
20219
20202
201911
201810